Volume 615, July 2018
|Number of page(s)||17|
|Section||Galactic structure, stellar clusters and populations|
|Published online||06 July 2018|
Combined dynamical effects of the bar and spiral arms in a Galaxy model. Application to the solar neighbourhood
Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, 05508-090 São Paulo, Brazil
e-mail: firstname.lastname@example.org; email@example.com; firstname.lastname@example.org
Accepted: 17 April 2018
Context. Observational data indicate that the Milky Way is a barred spiral galaxy. Computation facilities and availability of data from Galactic surveys stimulate the appearance of models of the Galactic structure, however further efforts are needed to build dynamical models containing both spiral arms and the central bar/bulge.
Aims. We expand the study of the stellar dynamics in the Galaxy by adding the bar/bulge component to a model with spiral arms introduced in one of our previous publications. The model is tested by applying it to the solar neighbourhood, where observational data are more precise.
Methods. We model analytically the potential of the Galaxy to derive the force field in its equatorial plane. The model comprises an axisymmetric disc derived from the observed rotation curve, four spiral arms with Gaussian-shaped groove profiles, and a classical elongated/oblate ellipsoidal bar/bulge structure. The parameters describing the bar/bulge are constrained by observations and the stellar dynamics, and their possible limits are determined.
Results. A basic model results in a bar of 2.9 kpc in length, with a mass of the order of a few 109M⊙ (which does not include the axisymmetric part of the bulge, which has a mass of about 1010M⊙). The size and orientation of the bar are also restricted by the position of masers with Very Long Baseline Interferometry (VLBI). The bar’s rotation speed is constrained to Ωbar < 50 km s−1 kpc−1 taking into account the allowed mass range.
Conclusions. We conclude that our basic model is compatible with observations and with the dynamical constraints. The model explains simultaneously the bulk of the main moving groups, associated here with the spiral corotation resonance, and the Hercules stream, associated with several inner high-order spiral resonances; in particular, with the 8/1 resonance. From the dynamical constraints on the bar’s angular speed, it is unlikely that the bar’s outer Lindblad resonance (OLR) lies near the solar circle; moreover, its proximity would compromise the stability of the local arm structure.
Key words: galaxies: spiral / Galaxy: kinematics and dynamics / solar neighborhood / methods: analytical / methods: numerical
© ESO 2018
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